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A gamma-ray flare of quasar CTA 26. / Mattox, J. R.; Hallum, J. C.; Marscher, A. P.; Jorstad, S. G.; Waltman, E. B.; Teräsranta, H.; Aller, H. D.; Aller, M. F.

в: Astrophysical Journal, Том 549, № 2 PART 1, 10.03.2001, стр. 906-914.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Mattox, JR, Hallum, JC, Marscher, AP, Jorstad, SG, Waltman, EB, Teräsranta, H, Aller, HD & Aller, MF 2001, 'A gamma-ray flare of quasar CTA 26', Astrophysical Journal, Том. 549, № 2 PART 1, стр. 906-914. https://doi.org/10.1086/319435

APA

Mattox, J. R., Hallum, J. C., Marscher, A. P., Jorstad, S. G., Waltman, E. B., Teräsranta, H., Aller, H. D., & Aller, M. F. (2001). A gamma-ray flare of quasar CTA 26. Astrophysical Journal, 549(2 PART 1), 906-914. https://doi.org/10.1086/319435

Vancouver

Mattox JR, Hallum JC, Marscher AP, Jorstad SG, Waltman EB, Teräsranta H и пр. A gamma-ray flare of quasar CTA 26. Astrophysical Journal. 2001 Март 10;549(2 PART 1):906-914. https://doi.org/10.1086/319435

Author

Mattox, J. R. ; Hallum, J. C. ; Marscher, A. P. ; Jorstad, S. G. ; Waltman, E. B. ; Teräsranta, H. ; Aller, H. D. ; Aller, M. F. / A gamma-ray flare of quasar CTA 26. в: Astrophysical Journal. 2001 ; Том 549, № 2 PART 1. стр. 906-914.

BibTeX

@article{3690c9d0c50c455997f0c7d7daa046f7,
title = "A gamma-ray flare of quasar CTA 26",
abstract = "During the first 3 years of the Compton Gamma Ray Observatory mission, the blazar CTA 26 was observed 10 times by EGRET and not significantly detected. We report an observation in 1995 when CTA 26 flared to a peak γ-ray flux of (4.9 ± 1.5) x 10-6 cm-2 s-1 (E > 100 MeV), the third brightest of all EGRET blazars. Following the γ-ray flare, extensive VLBA and single-dish radio observations were obtained. We find two components of a milliarcsecond jet moving with apparent transverse velocities of 12 ± 1 h-1 c, and 5 ± 2 h-1 c (H0 = 100 h km s-1 Mpc-1, q0 = 0.1). The position angle of VLBI components appears to change with time. The slowest VLBI component's motion is consistent with ejection at the time of the 1995 γ-ray flare. A weak radio flare is also seen in Mets{\"a}hovi millimeter radio monitoring data, peaking within weeks of the γ-ray flare.",
keywords = "Gamma rays: observations, Quasars: general, Quasars: individual (CTA 26), Radio continuum: general, Techniques: interferometric",
author = "Mattox, {J. R.} and Hallum, {J. C.} and Marscher, {A. P.} and Jorstad, {S. G.} and Waltman, {E. B.} and H. Ter{\"a}sranta and Aller, {H. D.} and Aller, {M. F.}",
year = "2001",
month = mar,
day = "10",
doi = "10.1086/319435",
language = "English",
volume = "549",
pages = "906--914",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2 PART 1",

}

RIS

TY - JOUR

T1 - A gamma-ray flare of quasar CTA 26

AU - Mattox, J. R.

AU - Hallum, J. C.

AU - Marscher, A. P.

AU - Jorstad, S. G.

AU - Waltman, E. B.

AU - Teräsranta, H.

AU - Aller, H. D.

AU - Aller, M. F.

PY - 2001/3/10

Y1 - 2001/3/10

N2 - During the first 3 years of the Compton Gamma Ray Observatory mission, the blazar CTA 26 was observed 10 times by EGRET and not significantly detected. We report an observation in 1995 when CTA 26 flared to a peak γ-ray flux of (4.9 ± 1.5) x 10-6 cm-2 s-1 (E > 100 MeV), the third brightest of all EGRET blazars. Following the γ-ray flare, extensive VLBA and single-dish radio observations were obtained. We find two components of a milliarcsecond jet moving with apparent transverse velocities of 12 ± 1 h-1 c, and 5 ± 2 h-1 c (H0 = 100 h km s-1 Mpc-1, q0 = 0.1). The position angle of VLBI components appears to change with time. The slowest VLBI component's motion is consistent with ejection at the time of the 1995 γ-ray flare. A weak radio flare is also seen in Metsähovi millimeter radio monitoring data, peaking within weeks of the γ-ray flare.

AB - During the first 3 years of the Compton Gamma Ray Observatory mission, the blazar CTA 26 was observed 10 times by EGRET and not significantly detected. We report an observation in 1995 when CTA 26 flared to a peak γ-ray flux of (4.9 ± 1.5) x 10-6 cm-2 s-1 (E > 100 MeV), the third brightest of all EGRET blazars. Following the γ-ray flare, extensive VLBA and single-dish radio observations were obtained. We find two components of a milliarcsecond jet moving with apparent transverse velocities of 12 ± 1 h-1 c, and 5 ± 2 h-1 c (H0 = 100 h km s-1 Mpc-1, q0 = 0.1). The position angle of VLBI components appears to change with time. The slowest VLBI component's motion is consistent with ejection at the time of the 1995 γ-ray flare. A weak radio flare is also seen in Metsähovi millimeter radio monitoring data, peaking within weeks of the γ-ray flare.

KW - Gamma rays: observations

KW - Quasars: general

KW - Quasars: individual (CTA 26)

KW - Radio continuum: general

KW - Techniques: interferometric

UR - http://www.scopus.com/inward/record.url?scp=0035835788&partnerID=8YFLogxK

U2 - 10.1086/319435

DO - 10.1086/319435

M3 - Article

AN - SCOPUS:0035835788

VL - 549

SP - 906

EP - 914

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART 1

ER -

ID: 88368054